arXiv:1606.01066v1 [astro-ph.SR] 3 Jun 2016 et) ón ta.(99 0 bet)adHja ta.(20 al. et Hajian ob- and 22 objects) (1998, 101 objects). al. (1999, 18 et al. Hua et object objects), Górny 243 19 jects), (1996, (1996, al. Kwitter et & Manchado Tweedy objects), 50 (1987, co Balick catalogues previous [N relevant the most studie taining The few objects. a of only addition, number [N In in type. observations this contain of works many not are the and (EABA). Alegre (CASLEO) Bosque Leoncito de El Astrofísica t Estación Astronómico like Complejo telescopes medium-sized the for whi of project time-consuming, ideal have is a an to complete work it as PNe, makes of is type of that this images study However, narrow-band a possible. of sample for a particular to access in and objects, nomical formation. PN in involved a ejection information mass provide of also processes the and mass ionized of context, distribution centred this images In narrow-band understood. di of atlas fully p complete yet mass-loss and not extensive the as are such which scheme cesses, evolutionary their of details o tr fbten08ad8M 8 ev and stellar 0.8 of between P stages of The latest un- the studied. for ago; of poorly decade representative remain a highly are still as are them many (PNe) as of nebulae twice most than fortunately, planetary more is Galactic which known, 3000 about Currently, Introduction 1. este fL lt,CroaadSnJuan. San and Nati Córdoba the Plata, and La Argentina of República versities la de Invest Técnicas de y Nacional Consejo Científicas the between agreement under ated etme 8 2018 18, September Astronomy ⋆ ff rn eua ie sesnilbcueteeiae trace images these because essential is lines nebular erent ept h motneo hs arwbn uvy,there surveys, narrow-band these of importance the Despite astro- extended about study any for important is it Clearly, iiigAtooe,Cmlj srnmc lLoct ope Leoncito El Astronómico Complejo Astronomer, Visiting .A Weidmann A. W. e words. Key vial nteltrtr,adbifl eciealcssi cases all describe briefly and literature, the in available rvddb hsalsrpeetoeo h otetnieim extensive most the of one represent atlas this Estació by the and provided (CASLEO), Leoncito El Astronómico Complejo le ete ntenblreiso fte[N the of o emission images nebular original the hundred on one centred than filter more of atlas an present We 2018 18, September 2 4 3 1 osj ainld netgcoe inícsyTécnicas y e-mail: Científicas Investigaciones de Nacional Consejo autdd aeáia srnmayFsc,UiesddN Universidad Física, y Astronomía Matemática, de Argentina Facultad Córdoba, 854, Laprida Uni (IATE), Córdoba, Experimental de y Teórica Astronomía de Instituto bevtroAtoóio nvria ainld Córdob de Nacional Universidad Astronómico, Observatorio & ta fmncrmtciae fpaeaynebulae planetary of images monochromatic of Atlas ii [email protected] Astrophysics arwbn hthv enpbihdaeby are published been have that band narrow ] lntr eua:Gnrl–Alss–Ctlg tr:mas Stars: – Catalogs – Atlases – General nebulae: Planetary 1 , 2, ⋆ ii n ngnrlcvrol small a only cover general in and ] .O Schmidt O. E. , aucitn.neb1 no. manuscript ⊙ oee,teeaesilmany still are there however, ; 3 .R eaValdarenas Vena R. R. , ii uigsvrlosrigcmagsuigtomoderate-ap two using campaigns observing several during ] Rsac Note) (Research nlUni- onal igaciones hc u [N our which n olution hose bout ABSTRACT 07, the Ne ro- on s), ch an g uvy fPei [N in PNe of surveys age n- (CONICET) esddNcoa eCroa OIE,Osraoi Astro Observatorio CONICET, Córdoba, de Nacional versidad r- ,Lpia84 00Croa Argentina Córdoba, 5000 854, Laprida a, lntr eua Pe.Teeiae eetkni narro a in taken were images These (PNe). nebulae planetary f s s coa eCórdoba de acional srfsc eBsu lge(AA,bt nAgnia Th Argentina. in both (EABA), Alegre Bosque de Astrofísica n l fojcs l fwihwr bevda o eihdista zenith low at observed sa were our show which (z summarizes of to all 4 Table oversaturated objects, . of purposely ob- ple the were of Some regions 2-15, acquired. faintest He were the as each such minutes jects, ten genera of lower in the exposures where, hand, CASLEO three other at the observed On were PNe. objects the brightness of most for obtained were shown are used filters EABA. the 1. at of Fig. describe curves 30 are transmission and systems to The observational CASLEO 1. 2013 Table the at of from nights features runs 7 main of observing The were total several survey a of m this making course for 2.15 2015, data the the over imaging and taken The focus) newtonian CASLEO. the at telescope in (configured EABA detec at to cases, some in be and, should it (LIS). morphology way, regions its low-ionization this In infer arcsec. to 200 mentione possible and the 16 criter in between selection objects quality be the Our the of alogues works. size compare previous angular to the of that chosen that requires was with that data our group Th of small (2005). a al. [N in et for observations the Parker previous cept from have and not selected (1992) did PNe nebulae al. selected true et 108 Acker of of sample catalogues a observed have We reduction data and observations, Sample, 2. will ones) previous research. the future for with database (together useful work a become this that obje complex hope highly We and amazing these of data observational [N the < ii 40 nEB,sre f2 osctv i-iueexposures six-minute consecutive 20 of series EABA, In telescope m 1.54 the obtained were data observational The in PNe 108 comprising images of atlas an present we Here mgsrva e n neetn structures. interesting and new reveal images ] 3 ◦ s-loss .A Ahumada A. J. , ). ii arwbn.Tega st nraeteaon of amount the increase to is goal The band. narrow ] ii .W opr h e mgswt those with images new the compare We ]. 1 .G Volpe G. M. , ruetlsoe,a the at telescopes, erture ril ubr ae1o 36 of 1 page number, Article 1 n .Mudrik A. and

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Table 1. Summary of the main features of the observational systems.

EABA filter EABA CASLEO CASLEO filter telescope size [m] 1.54 2.15 f-ratio 4.9 8.6 CCD brand Apogee Roper detector size [px] 3072 × 2048 2048 × 2048 binning [px] 3 × 3 5 × 5 pixel scale [arcsec/px] 0.74 0.75 field of view [arcmin] 12 × 8 5.1 × 5.1 central λ [Å]a 6578 6582 [%] Transmission bandpass filter [Å]a 20 18 filter transmission Tλ6585 0.92 0.53 zero-point k0 [mag] −3.38 ± 0.10 −1.77 ± 0.03 ff / − ± − ± ext. coe . k1 [mag airmass] 0.08 0.04 0.11 0.02 0 20 40 60 80 100 −2 6540 6560 6580 6600 6620 lim. magnitude [mag arcmin ] 12.1 12.6 ° Wavelength [A] Notes. The default gain for each instrument was used in all runs. (a) see Fig. 1. Fig. 1. Effective transmission curves for the filters (at 20 degrees Cel- sius). Image reduction was performed using standard procedures with IRAF1. Thus, the data were first trimmed, bias-subtracted using a series of ten averaged bias frames and dark-subtracted (only in frames of EABA). The data were then flatfielded using a series of twilight flat fields. After the reduction was complete, the individualframes were spatially aligned to a common system using the IRAF task imalign. Typically, four stars were used to obtain this transformation. After that, all images were combined, cosmic rays removed, and the signal-to-noise (S/N) improved (IRAF task imcombine). Finally the images were rotated so that north was up and east to the left (IRAF tasks imtranspose and rotate).

The sky conditions during each night varied greatly. The Normalized Frequency combined effects of occasional poor telescope guiding and vari- able dome and sky seeing resulted in the stellar FWHM ranging from 2′′ to 5′′, as illustrated in Fig. 2 for CASLEO. Moreover, since the final images suffered a slight degrada- tion in quality due to the spatial alining process, this effect is 0.002.0 0.05 0.102.5 0.15 0.20 0.25 3.0 3.5 4.0 shown in Fig. 2. The combined images with a seeing greater than Seeing [arcsec] 4′′ were rejected. All the objects in the atlas have a S/N > 4. More details about the images that were obtained at EABA are reported in Vena Valdarenas et al. (2015). Fig. 2. FWHM of stars in CASLEO images, measured in the final com- bined frame (green) and individual reduced images (red).

2.1. Photometric calibration and detection limit 600 seconds of PN G242.5−05.9 at airmasses of ∼1.01, and of To assess the detection limit at each observatory, two additional 360 seconds at ∼1.15 for PN G002.7−52.4 were obtained and nights were devoted to the observation of two planetary nebu- combined to improve the S/N relation. lae and of a number of spectrophotometric standard stars to first Aperture photometry was performed on nebulae and stars derive the extinction coefficients for the filters and the sensibil- with the package daophot in IRAF. For standard stars, aper- ity of the instrumental systems. The observed nebulae are i) the tures with radii of four times the FWHM of the stellar im- faint PN G242.5−05.9(on the night of 15–16October 2015 from ages were adopted without recourse to aperture correction. For CASLEO), and ii) the brighter PN G002.7−52.4(IC 5148,on the PN G242.5−05.9 an aperture of 30 arcsec of radius centred on night of 17–18 October 2015 from EABA). During each night, α = 07h26m04s.9, δ = −28◦58′23′′.6 (J2000.0) was used, and for several secondary and tertiary spectrophotometric standard stars PN G002.7−52.4 an aperture of 79 arcsec of radius centred on from Hamuy et al. (1994) were also observed at airmasses in the α = 21h59m35s.1, δ = −39◦23′07′′.1 (J2000.0) was chosen. In ranges 1.01–1.88 (CASLEO) and 1.01–1.41 (EABA). Exposures the first case, four stars that appear inside the nebula and a fifth for the stars reach from a few to 180 seconds. Several images of one very near its apparent limits were successfully subtracted before performing the photometry. No was subtracted from 1 IRAF: the Image Reduction and Analysis Facility is distributed by the National Optical Astronomy Observatories, which is operated by the IC 5148. Association of Universities for Research in Astronomy, Inc. (AURA) The transformation equations are of the form: under cooperative agreement with the National Science Foundation (NSF). M(λ6585) = m(λ6585) + k0 + k1 × X, (1)

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Table 2. Adopted magnitudes at λ6585 of spectrophotometric stan- It must be pointed out, finally, that the transformation de- dards. rived in this section is in general not applicable to our collection of images, since observing on photometric nights was not a re- Star M(λ6585) quirement for the original purposes of this work. EG21 11.936 HR718 4.611 3. Considerations about the survey HR1544 4.634 HR9087 5.414 3.1. Narrow-band filters LTT377 11.106 LTT 1020 11.320 When interference filters are used in a converging beam, the pri- LTT 2415 12.125 mary effect is a shift of the transmittance peak towards shorter wavelengths (Eather & Reasoner 1969). Table 3. Calibrated magnitudes and fluxes at λ6585 of two planetary Another important phenomenon that affects our observations nebulae. is the bandpass shift due to variations of the ambient temperature (Pogge 1992). It moves towards the red or the blue, depending PN G002.7−52.4 PN G242.5−05.9 on whether the temperature increases or decreases, respectively, (EABA) (CASLEO) following a linear temperature dependence. For a narrow-band filter, the shift in mean wavelength due to temperature is about M(λ6585) 8.78 ± 0.04 14.20 ± 0.12 0.18Å per degree Celsius. An additional problem is posed by the a −13 −15 fλ (7.8 ± 0.3) × 10 (5.2 ± 0.6) × 10 age of filters: after 6-10 years they usually deteriorate, mainly log fλ −12.11 ± 0.04 −14.3 ± 0.1 losing transmittance. surface brightnessb 10.36 ± 0.05 12.56 ± 0.14 On the other hand, we have to take into account the radial surface brightnessc (5.0 ± 0.6) × 10−17 (6.6 ± 1.0) × 10−18 velocity of the objects. The of a PN could cause the [N ii] emission to falls outside of the effective bandpass of Notes. (a) erg cm−2 s−1Å−1. (b) mag arcmin−2. (c) erg cm−2s−1Å−1arcsec−2. the filter. Unfortunately, many objects included in our atlas do not have radial velocity determinations, in particular the objects extracted from the MASH catalogue (Parker et al. 2005). where M(λ6585) is the calibrated monochromatic magnitude at The filter peak transmittance was determined at a tempera- λ6585, m(λ6585) is the instrumental magnitude with an arbitrary ture of 20◦C, which means that those objects that were observed zero point of 21.0, k and k are the zero-point and extinction co- 0 1 from EABA in winter (where the temperature may drop to 5◦) efficients, and X is the airmass. It is worth mentioning that the and with positive radial velocity might be contaminated by Hα system sensitivity, including the effects of telescope optics and emission. These objects are labelled in Table 4, where we used detector response, and the filter transmission at λ6585 (T , λ6585 the radial velocity data from Durand et al. (1998) as a reference. listed in Table 3), are included in k . The values of M(λ6585) for 0 Finally, it is necessary to consider another possible nebular the observed spectrophotometric standards were obtained by in- emission in this wavelength range. Fortunately, there are only terpolatingin Tables 6 and 7 ofHamuyet al. (1994)and arelisted ii in Table 2. The derived coefficients and their errors, as given by very few nebular lines (C at 6578.05 and 6582.88Å) that could daophot, are given in Table 1. The monochromatic magnitudes contaminate our data. Nevertheless, contamination by continu- of the nebulae are shown in Table 3; these are related to the flux ous nebular emission will always be present. density fν at λ6585 by 3.2. Comparison with other observations M(λ6585) = −2.5 × log10( fν) − 48.590, (2) −2 −1 −1 Our work has objects in common with the catalogues of Balick (Hamuy et al. 1994), where fν is expressed in erg cm s Hz . This flux density has to be multiplied by the factor c/(6585)2 (1987) and Hua et al. (1998). These objects are labelled in Ta- ble 4. With the former,the only nebula in common is NGC 2610, (c is the speed of light) to give it as fλ, that is, in the units erg cm−2 s−1 Å−1. After propagating the errors adequately, the which we observed from EABA. In this case the Balick images flux densities of the nebulae and their logarithms are those listed are deeper. in Table 3. Our atlas includes ten PNe that were observed by Hua et al. ffi The surface brightnesses were calculated by adopting for cir- (1998). The comparison in this case is more di cult, since Hua ff cular shapes and areas of 0.217 arcmin2 (PN G242.5−05.9) and used three di erent telescopes and we used two. However, the 4.313 arcmin2 (PN G002.7−52.4) for the nebulae. For the first, images of those PNe that were observed from CASLEO are of a surface brightness of 12.56 mag arcmin−2 ataS/N ∼ 4 for an a quality and depth comparable to those obtained by Hua et al. exposure time of 600 seconds is estimated, while for IC 5148 (1998) (e.g. He 2-70 and K 1-3). the value is 10.36 mag arcmin−2 with S/N ∼ 20 and 360 sec- onds. These brightnesses, expressed in magnitudes per squared 4. Notes on individual objects arcmin and also in erg cm2 s−1 Å−1 arcsec−2, are listed in Ta- ble 3. While the surface brightness of the faint nebula observed PN G002.7−52.4: ring-like PN with an inner highly elongated at CASLEO can be adopted as the limiting magnitudefor the im- elliptical ring with several irregularities in the brightness and an ages taken there, IC 5148 is rather bright, therefore we divided external round fainter nebulosity. More images can be found in its flux by 5 to obtain a S/N relation of ∼ 4 like that measured Streicher (2010), Moreno et al. (1991), and Chu et al. (1987). in a combination of 360-second exposures of the faint nebula PN G003.1+02.9: Stanghellini et al. (1993a) classified this Hf 39 (Figure 13). The magnitude calculated with this new flux, PN as irregular. We disagree with this classification because in 12.1 mag arcmin−2, can now be considered as the limiting mag- our image we can see an elliptical structure with prominent jets. nitude in the images obtained at EABA for this survey. More images can be found in Miszalski et al. (2009), López

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(2000), Zhang & Kwok (1998), Hajian et al. (1997), López et al. low surface brightness towards the NE and a emission region to- (1997), and Corradi et al. (1996). wards the SSE that is difficult to explain. It probably is a bipolar PN G013.8−02.8: bipolar PN. More images can be found in PN. This object requires a more detailed study. Saurer & Weinberger (1987). PN G258.0−15.7: Gonçalves et al. (2002) show an [N ii] im- PN G014.8−25.6: faint nebulosity with no obvious symme- age, but it is not as deep as ours. In both cases the huge jet-like try. features are clearly visible. Additional images can be found in PN G019.4−13.6: middle elliptical according to the morpho- Corradi et al. (1996) and Corradi et al. (1999). logical scheme of Balick (1989). More images can be found in PN G259.1+00.9: it is difficult to perform a morphological Bohigas (2003). classification of this Type I PN. A complete analysis of this ob- PN G043.5−13.4: PN with no clear symmetry, roughly ellip- ject was made by Jones et al. (2014). Our [N ii] image does not tical with a nearly rectangular shape. More images can be found show any differences with the [N ii]+Hα published in that article. in Schwarz et al. (1992). AHα image is presented by Górny et al. (1999). PN G118.8−74.7: a bright and well-studied object. Phillips PN G260.7−03.3: the Hα image of MASH catalogue dis- (2003) classified this PN as round. Our image shows that it has plays a more extended HII region than our image. According to an elliptical shape with an inner filamentary structure and intense its morphology,it wouldnotbe a PN. Itcouldbe a filamentof the patches to the SE. We suggestthat theobject needsto bereclassi- supernova remnant (SNR) Puppis A (Goudis & Meaburn 1978). fied. Images of this object are found in Pereyra et al. (2013), Chu PN G261.6+03.0: Corradi & Schwarz (1995) classify this et al. (2009), Hoogerwerf et al. (2007), Moore (2007), Szentgy- Type I PN as a possible/probable bipolar. Our [N ii] image shows orgyi et al. (2003b), and Szentgyorgyi et al. (2003a). a well-defined bipolar morphology with a pronounced waist, PN G209.1−08.2: in the MASH images the object is very thus we confirm this classification. It is not evident from our faint and does not reveal any morphology. In our image it shows image if the two saturated regions define the torus of the waist. a clearly round morphology, with non-uniform brightness. If this were the case, the waist would not be perpendicular to the PN G215.6+11.1: curious morphology, nebula with a nearly bipolar lobes. To answer this question, it is necessary to perform rectangular shape. Possible bipolar PN. a detailed spectroscopic study. PN G217.2+00.9: probable interaction with the ISM. PN G261.9+08.5: this Type I PN has been classified by Pe- PN G224.3−03.4: probable interaction with the ISM. imbert & Torres-Peimbert (1983) as a filamentary bipolar. More PN G225.4+00.4: intriguing morphology, it displays a non- images can be found in Vázquez (2012), Bohigas (2003) and concentric multishell, similar to the mysterious rings of super- Dufour (1984). nova 1987A. PN G262.6−04.6:it presents a roughly round shape with two PN G226.7+05.6: all authors agree that the object shows a intense oval patches. Additional images can be found in Long- bipolar morphology. Stanghellini et al. (1993b) classified it as more & Tritton (1980) and Schwarz et al. (1992). bipolar with an outer structure. More images can be found in PN G263.3−08.8: this object does not have published Huggins et al. (2000), Perinotto & Corradi (1998), Corradi & narrow-bandimages. Our image shows a roundmorphologywith Schwarz (1995), Schwarz (1992), Schwarz et al. (1992), and a dark band crossing the core, with a PA of 135◦. Additional im- Corradi & Schwarz (1993a). ages can be found in Fredrick & West (1984). PN G233.0−10.1: ring-like PN. More images can be found PN G264.1−08.1: well-defined elliptical nebula with a high in Saurer & Weinberger (1987). surface brightness and an evident central star. PN G236.0−10.6: object poorly studied, morphology type PN G265.1−04.2:ring-like PN with some knots on the edge. one-side (see Ali et al. 2000) with radial filaments. More images It is unclear if the off-centre bright star is indeed its ionizing can be found in Hartl & Weinberger (1987). source. Additional images can be found in Fredrick & West PN G236.7−01.6: our image shows two areas of lower (1984). brightness that are not visible in the Hα image of the MASH PN G265.4+04.2: round PN with two diametrically opposed catalogue. condensations. Probable bipolar PN. PN G239.6−12.0: round with internal structure and intense PN G268.6+05.0: object with no obvious symmetry. It dis- patches. More images can be found in Fredrick & West (1984). plays an oval ring-like internal structure with opposite faint PN G239.6+13.9: Balick (1989) classified this PN as ellip- ansae. It might be a bipolar PN. tical (early-middle subtype). Additional images can be found in PN G268.9−00.4: this fascinating object has the appearance Schwarz et al. (1992). of a steering wheel. There is a nebulosity in the NW that is not PN G243.8−37.1: Boffin et al. (2012a) performed a morpho- visible in the MASH Hα image. It is unclear if it belongs to the logical analysis of this PN. nebula. The central bright star could be the ionizing source. This PN G247.5−04.7:there is an HII region towards the SW, and object deserves a more detailed study. it is unclear whether it is part of the PN or is the optical counter- PN G274.6+03.5:roundPN with a bright bar along its diam- part of the molecular cloud BRAN 63. eter. Additional images can be found in Górny et al. (1999). PN G249.3−05.4: ring-like PN with a very faint CSPN. It PN G276.1−03.3: object that probably has a double enve- shows several irregularities in the brightness of the ring. lope. PN G249.8+07.1: this seems to be two overlapping PN. It is PN G277.1−03.8:López et al. (1989) have classified this PN difficult to explain the homogeneous and extensive overdensity as an evolved bipolar, but Louise et al. (1987) have classed it of material towards the NW. as peculiar. It has an overall bow-shock morphology, which was PN G250.4−01.3: classical bipolar PN with an arc towards also noted by Rauch et al. (1999). Perhaps the gaseous envelope the NW. It is also visible in the [N ii] images of Kerber et al. has interacted with the ISM. A detailed analysis of this object (2000). was presented by (Lopez et al. 1991). More narrow-band images PN G257.5+00.6: poorly studied with in- can be found in Drew et al. (2014), Perinotto & Corradi (1998), triguing morphology. The PN displays a ring-like structure of Corradi & Schwarz (1995), and (Lopez et al. 1991).

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PN G277.7−03.5: a round morphology with a complex ion- PN G302.6−00.9: object poorly studied even though it dis- ization structure was revealed in our image. This object deserves plays a curious morphology. The PN exhibits an elliptical ring- a more detailed study. like main structure. It seems to have a pair of symmetric jets in PN G278.5−04.5: this object has been very poorly studied. PA=135◦. Our image shows an elliptical envelope with an internal structure PN G304.2+05.9: a ring-like object with a strange arc to- of point-symmetric type. In addition, we observe two pairs of wards the NW. This is a very poorly studied object, it requiresa beams in the E-W direction, similar to those of the Egg nebulae. more detailed analysis. PN G279.1−03.1: roughly elliptical with two knots diamet- PN G307.2−03.4:PN with a puzzlingmorphologyand a very rically opposed. hot [WO1] central star. Phillips & Reay (1983) reported five sets PN G279.6−03.1:bipolar (Corradi & Schwarz 1995), intense of ansae, but Reay et al. (1984) described this situation as a ring knots are superimposed at each end of the minor axis. In addi- of condensations. Zuckerman & Aller (1986) classified this PN tion, it has a pair of arcs that make it an S-shaped nebula (Lee as irregular (with condensations and filaments), but Corradi & et al. 2007b). A detailed study of this object has been made by Schwarz (1995) classified it as a probable or possible bipolar PN Corradi & Schwarz (1993b). More images can be found in Lee and Pascoli (1990) as a late butterfly. Finally, Sabin et al. (2012) et al. (2007a), Perinotto & Corradi (1998) and Schwarz et al. performed a detailed study of this object and classified it as a (1992). quadrupolar nebula with multiple sets of symmetrical condensa- PN G280.0+02.9: round or point-like nebula. We do not de- tions. Moreover, a spherical halo is evident in the [O iii] image tect any outer structure. presented by Hua et al. (1998). In our image we can distinguish PN G285.5−03.3: strange morphology for a PN. Perhaps it two mass-loss events. The first is an irregular structure of intense is indeed the LEDA 2792457 and/or LEDA 2792455. knots, and the other is an internal and discontinuous bar. More PN G286.3−00.7: Smith et al. (2007) showed a [N ii]+Hα images can be foundin Górnyet al. (1999),Polcaro et al. (1997), narrow-band image of this PN. It is a clear ring PN. Perinotto et al. (1994), and Greve & van Genderen (1987). PN G286.3+02.8:ring-like PN with a bright condensation to PN G309.0−04.2: we agree with the morphological descrip- the SW. tion of Stanghellini et al. (1993a), who classified it as an ellipti- PN G288.4−01.8: bipolar, it seems that its waist is a torus. cal with internal structure. Moreno et al. (1991) reported a neb- PN G288.4+00.3: it probably has two symmetrical jets at PA ulosity to the NW that we do not see. More images can be found 100◦. in Kaler et al. (1989) and Schwarz et al. (1992). PN G288.9−00.8: possible WR star of population I (Smith PN G309.2+01.3: this PN is interacting with the ISM (Ali et al. 1994). Additional images can be found in Stahl (1987) and et al. 2012). Frew et al. (2014). PN G310.7−02.9: narrow-band images are provided in PN G290.1−00.4: clear bipolar morphology with an bright Górny et al. (1999) and Moreno et al. (1991). waist. Moreover, in our image two ansae perpendicular to the PN G310.8−05.9: round PN. More narrow-band images are minor axis are evident, which are not clear in the image pub- shown in Longmore & Tritton (1980). lished by Hua et al. (1998). PN G311.7−00.9: bipolar, the waist looks like a torus. The PN G290.5+07.9: the central star is visible. Well-studied ob- central star is evident. ject (see Palmer et al. 1996; Lopez et al. 1993), deeper images PN G315.0−00.3: the Hα image from Górny et al. (1999) can be found in Boffin et al. (2012b). shows a condensation towards the NW that is not visible in our PN G292.6+01.2: very bright PN with a complex internal image. Other images are presented by Moreno et al. (1991), structure. Bipolar appearance with a faint external shell. More Meaburn & Walsh (1989), and Moreno et al. (1987). images can be found in Górny et al. (1999). PN G317.1−05.7: the MASH Hα image shows an external PN G293.6+01.2: possible bipolar, with a very brilliant envelope that is not visible in ours. On the other hand, the Hα waist. image (Moreno et al. 1991) does not reveal the internal structure PN G293.6+10.9: well-defined irregular disc with a central that appears in our [N ii] image. In the [O iii] image (Górny et al. hole. A double-shell structure can be seen. Aditional images can 1999) none of these structures are visible. Other narrow-band be found in Rauch et al. (1999). images can be found in Moreno et al. (1987). PN G294.6+04.7: very complex object that has been studied PN G317.8+03.3: poorly studied PN that presents a ring-like in detail. It shows jets and knots (Corradi et al. 1999), an ex- inner structure with several irregularities in the brightness. A dif- tended halo (Corradi et al. 2003, 2004), and a bow-shock feature fuse nebulosity is superimposed at each end of the minor axis. (Guerrero et al. 2013). Additional narrow-band images can be PN G318.3−02.0: all authors agree with the classsification found in Schwarz et al. (1992) and Richer et al. (1991). of this PN as bipolar. More images can be found in Górny et al. PN G294.9−00.6: round morphology, an exterior elliptical (1999), Corradi & Schwarz (1995), Moreno et al. (1991), Louise structure may be present (PA=0◦). The central region is probably et al. (1987), and Moreno et al. (1987). obscured by dust. PN G318.3−02.5: well-defined elliptical nebula with two in- PN G296.6−20.0: elliptical morphology that resembles the tense patches. More images can be found in Górny et al. (1999), Owl nebula. Moreno et al. (1991), and Moreno et al. (1987). PN G298.2−01.7: Corradi & Schwarz (1995) classified it as PN G318.4−03.0: ring-like PN. a probable or possible bipolar PN. Our image allows us to con- PN G319.6+15.7: Type I PN with a [WR] core. This PN, firm this classification. More images can be found in Górny et al. according to its appearance, is a typical bipolar, but Zuckerman (1999). & Aller (1986) described this object as a disc of approximately PN G299.0+03.5: roughly elliptical with a bright waist. The uniform brightness, elliptical shape, and ansae. Hua et al. (1998) central star is evident. reported some internal structures. Several images of this PN have PN G299.0+18.4: ring-like with a diffuse double-shell; the been taken in multiple works, for example O’Dell et al. (2002), central star is visible. Additional narrow-band images can be Zhang & Kwok (1998),Corradi & Schwarz (1995),and Schwarz found in Schwarz et al. (1992). et al. (1992).

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PN G321.8+01.9: ring-like type with a clear ansae to the W. with intense knots that are superimposed at each end of the mi- Moreover, two symmetric condensations towards N and S are nor axis. In addition, this object has an outer shell structure that visible. We classify this object as a PE according to the classi- is not perpendicular to the former. Hua et al. (1998) suggested fication scheme of Gorny et al. (1997). On the other hand, this that it is a bipolar PN, but we are unable to confirm this asser- PN has been classified as elliptical by Phillips (2003).Additional tion. narrow-band images can be found in Górny et al. (1999). PN G352.9+11.4: round PN with a [WCL] core. The mor- PN G322.4−02.6: in the [N ii]+Hα image published by phology of this objects together with its brilliant CSPN make it Marston et al. (1998), the knots at the edge of the object towards similar to a nebula around a WC star of population I. Additional the NW are not visible, but they are clear in our [N ii] image images can be found in Schwarz et al. (1992). and may be LIS. Hα and [N ii] images shown by Schwarz et al. PN G353.7−12.8: this object could be the galaxy (1992) are overexposed. They do not show the complex internal IRAS 18232−4031 according to its spiral morphology. structure that is evident in our [N ii] image. PN G327.8−07.2: the Hα image shows an elliptical ring of a 5. Results faint nebulosity (Moreno et al. 1991). Our [N ii] image is similar to the [O iii] image of Moreno et al. (1991), showing a disc-like The atlas of monochromatic images is presented in Figs. 3 to PN. In addition, a faint nebulosity to the N and S of the inner 20. In all the images we tried different brightness and contrast region is visible in both images. levels to emphasize the most interesting features of each object. PN G328.9−02.4: round PN, the diffuse nebulosity to the S A logarithmic scale is indicated with an “(L)” in the caption of that we see in our imageis not visible in the [O iii] images shown the figures. by Górny et al. (1999). It may be an ultracompact HII region Our atlas includes objects that do not have any morpholog- (Walsh et al. 1997). There is a young stellar object candidate ical classification (e.g. Wray 16−20, ESO 259−10, LoTr 7, and near to this object, reinforcing the hypothesis of an HII region. VBRC 6) or are very poorly studied (e.g. HaWe 9, SaWe 1, PN G329.3−02.8:the Hβ image (Górny et al. 1999) does not ESO 427−19, and ESO 209−15); in particular, it contains im- show the two arcs (N and S) visible in our [N ii] image. This ages of recently classified PNe (Parker et al. 2005). Moreover, structure could be a LIS. The central star is not at the geometric this catalogue shows and reveals very interesting structures in centre, probably because of an interaction with the ISM. several nebulae. For example, PHR0716−1053 displays a non- PN G331.5−03.9: elliptical shape with internal structures. concentric multishell, resembling the mysterious rings of super- Additional images can be found in Górny et al. (1999). nova 1987A, or the outstanding planetary nebulae VBRC 1 and PN G332.0−03.3: round shape with several irregularities in Wray 16−121that shows a capricious distribution of ionized ma- the brightness. Additional images can be found in Górny et al. terial. (1999). We compared our images with those available in the litera- PN G334.3−09.3: Gorny et al. (1997) classified this object ture (even if they were taken in another filter), to compare our as a bipolar PN, subclass BE, and we agree with this classifi- classification morphology with previous ones given by other au- cation. On the other hand, Stanghellini et al. (1993a) classified thors. As a result, we reclassified some objects and provided one it as elliptical with outer structure. The Hα image published by to those nebulae that did not have previous classification. Schwarz et al. (1992) shows a round halo. We hope that these new images and morphological descrip- PN G340.8+10.8: diffuse nebulosity, elliptical shape. Two tions presented here will provide a guide for future research, thus symmetric arcs are easily discernible superimposed at the edge contributing to a better understanding of the final stages of stellar of the nebula (PA=70◦). This feature is not evident in the Hα evolution. image published by Górny et al. (1999). Acknowledgements. We thank the referee, Romano Corradi, whose very useful PN G341.8+05.4: our image is different from the Hα image remarks helped us to improve this paper. This work is partially supported by CONICET (PIP 11220120100298). The CCD and data ac-quisition system at published by Górny et al. (1999), perhaps because of the seeing CASLEO has been financed by R. M. Rich through U.S. NSF grant AST-90- effects. It is difficult to perform a morphological classification, 15827. This work is partially based on observations obtained with the 1.54m although it displays an elliptical shape (Gorny et al. 1997). We telescope of the Estación Astrofísica de Bosque Alegre, dependent of the Uni- can distinguish in our image an internal structure. More images versidad Nacional de Córdoba, Argentina. This research has made use of SAO Image DS9, developed by Smithsonian Astrophysical Observatory. This research can be found in Liu et al. (2000) and Pottasch et al. (1986). made use of the SIMBAD database, operated at the CDS, Strasbourg, France. PN G342.7+00.7: it is probably a bipolar PN. PN G342.9−02.0:the Hα image (Górny et al. 1999) displays a double-shell nebulosity. We can see in our [N ii] image that there is an arc towards the S, still far away from the nebula. References PN G342.9−04.9: this object shows a morphology similar to Acker, A., Marcout, J., Ochsenbein, F., et al. 1992, The Strasbourg-ESO Cata- PM 1-242 (Miranda et al. 2009).Additional images can be found logue of Galactic Planetary Nebulae. Parts I, II. in Górny et al. (1999). Ali, A., El-Nawawy, M. S., & Pfleiderer, J. 2000, Ap&SS, 271, 245 Ali, A., Sabin, L., Snaid, S., & Basurah, H. M. 2012, A&A, 541, A98 PN G345.4+00.1: ring-like internal structure, with an exter- Balick, B. 1987, AJ, 94, 671 nal faint shell, intense condensations are superimposed towards Balick, B. 1989, in IAU Symposium, Vol. 131, Planetary Nebulae, ed. S. Torres- the SE, and we can distinguish a knot towards the NE in our Peimbert, 83–92 image. Stanghellini et al. (1993a) classified it as elliptical with Boffin, H. M. J., Miszalski, B., & Jones, D. 2012a, A&A, 545, A146 Boffin, H. M. J., Miszalski, B., Rauch, T., et al. 2012b, Science, 338, 773 an internal structure, Gorny et al. (1997) classified it as a proba- Bohigas, J. 2003, Rev. Mexicana Astron. Astrofis., 39, 149 ble elliptical. Additional images can be found in Schwarz et al. Chu, Y.-H., Gruendl, R. A., Guerrero, M. A., et al. 2009, AJ, 138, 691 (1992). Chu, Y.-H., Jacoby, G. H., & Arendt, R. 1987, ApJS, 64, 529 + Corradi, R. L. M., Manso, R., Mampaso, A., & Schwarz, H. E. 1996, A&A, 313, PN G346.9 12.4: taking into account the peculiar morphol- 913 ogy of this bright nebula, it is surprising that it has been very Corradi, R. L. M., Perinotto, M., Villaver, E., Mampaso, A., & Gonçalves, D. R. poorly studied. It consists of a bright ring-like internal structure 1999, ApJ, 523, 721

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Fig. 3. [N ii] images of planetary nebulae. North is up and east to the left. The scale is indicated by a bar representing 60 arcseconds. From left to right, top IC 5148−50 and Hb 4 (L), middle SaWe 3 and HDW 12, bottom DeHt 3 and A 66.

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Fig. 4. Same as Fig. 3, top A 67 and NGC 246 (L), middle PHR0615−0025 (L) and K 1−11 , bottom PHR0702−0324 (L) and PHR0705−0924 (L).

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Fig. 5. Same as Fig. 3, top PHR0700−1143 (L) and PHR0716−1053, middle PHR0711−1238 (L) and M 1−6, bottom PHR0719−1222 (L) and PHR0727−1259 (L).

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Fig. 6. Same as Fig. 3, top PHR0727−1707 (L) and PHR0724−1757, middle SaWe 1 and HaWe 9, bottom PHR0730−2151 and ESO 427−19 (L).

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Fig. 7. Same as Fig. 3, top NGC 2610 and PHR0726−2858, middle PRTM 1 and PHR0742−3247, bottom A 23 and PHR0834−2819 (L).

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Fig. 8. Same as Fig. 3, top PHR0803−3331 (L) and PHR0736−3901, middle PHR0820−3516 and VBRC 1, bottom Wray 17−1 and He 2−11 (L).

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Fig. 9. Same as Fig. 3, top Wray 16−20 and He 2−15, middle NGC 2818 (L) and Wray 17−18 (L), bottom ESO 209−15 and He 2−7.

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Fig. 10. Same as Fig. 3, top ESO 259−10 and PHR0911−4205, middle PHR0927−4347 and PHR0905−4753, bottom He 2−37 and PHR0924−5506.

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Fig. 11. Same as Fig. 3, top NGC 2899 (L) and PHR0958−5039, middle Wray 17−31 and He 2−32 (L), bottom PHR0940−5658 and PHR1010−5146.

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Fig. 12. Same as Fig. 3, top He 2−36 (L) and Ste 2−1, middle PHR1019−6059 (L) and PHR1036−5909, bottom He 2−55 and PHR1046−6109.

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Fig. 13. Same as Fig. 3, top Hf 38 (L) and PHR1058−5853 (L), middle Hf 39 and Hf 48 (L), bottom Fg 1 (L) and NGC 3699 (L).

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Fig. 14. Same as Fig. 3, top He 2−70 and BlDz 1, middle NGC 3918 and He 2−72, bottom NGC 3195 (L) and He 2-76.

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Fig. 15. Same as Fig. 3, top PHR1221−5907 and K 1−23, middle Wray 16−121, and PHR1250−6346, bottom Wray 16−122 and NGC 5189 (L).

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Fig. 16. Same as Fig. 3, top He 2−99 (L) and VBRC 5, middle He 2−103 (L) and LoTr 7, bottom PHR1408−6229, and He 2−111 (L).

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Fig. 17. Same as Fig. 3, top He 2−119 (L) and VBRC 6, middle He 2−114 and He 2−116 (L), bottom ESO 135−04 and IC 4406 (L).

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Fig. 18. Same as Fig. 3, top He 2−120 (L) and Mz 1 (L), middle He 2−163 and He 2−146, bottom Mz 2 (L) and PHR1557−5128.

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Fig. 19. Same as Fig. 3, top He 2−165 (L) and He 2−164, middle IC 4642 (L) and Lo 12, bottom NGC 6153 and H 1−3.

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Fig. 20. Same as Fig. 3, top Pe 1−8 (L)and He 2−207, middle IC 4637 (L) and K 1−3, bottom K 2−16 (L) and Wray 16−411.

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Table 4. List of PNe included in our atlas. The PNe are denoted by their common name and by their PN G designation. Sixth column lists the telescope used in each observation, EABA and CASLEO, indicated by “E” and “C” respectively. Seventh column lists the number of combined images and eighth column shows the figure number for each nebulae. PNe observed by Hua et al. (1998) and Balick (1987) are marked by “*” and objects labelled with “†” have probably Hα contamination or only the continuum emission is detected.

N Name PNG RA(J2000) Dec(J2000) Telescope Images Figure 1 IC5148−50∗† 002.7−52.4 215931.7 −392236.2 E 10 3 2 Hb4 003.1+02.9 174152.7 −244208.0 E 11 3 3 SaWe 3∗† 013.8−02.8 182603.1 −181205.6 E 15 3 4 HDW12 014.8−25.6 195813.2 −262815.4 C 3 3 5 DeHt3 019.4−13.6 191704.6 −180134.2 E 17 3 6 A66 019.8−23.7 195731.8 −213636.8 C 8 3 7 A67 043.5−13.4 195829.3 +030222.6 C 3 4 8 NGC246∗ 118.8−74.7 004703.8 −115221.6 C 3 4 9 PHR0615−0025 209.1−08.2 061520.4 −002549.1 C 3 4 10 K1−11 215.6+11.1 073607.7 +024217.2 C 8 4 11 PHR0702−0324 217.2+00.9 070234.2 −032434.9 C 3 4 12 PHR0705−0924 222.9−01.1 070551.4 −092411.2 C 4 4 13 PHR0700−1143 224.3−03.4 070005.8 −114350.9 C 5 5 14 PHR0716−1053 225.4+00.4 071608.0 −105306.0 C 6 5 15 PHR0711−1238 226.4−01.3 071143.3 −123803.1 C 6 5 16 M1−16 226.7+05.6 073718.9 −093848.1 E 10 5 17 PHR0719−1222 227.1+00.5 071946.7 −122246.9 C 3 5 18 PHR0727−1259 228.6+01.9 072749.0 −125930.1 C 3 5 19 PHR0727−1707 232.1−00.1 072708.3 −170714.2 C 5 6 20 PHR0724−1757 232.6−01.0 072443.4 −175751.1 C 3 6 21 SaWe1 233.0−10.1 065041.0 −222609.3 C 3 6 22 HaWe9 236.0−10.6 065429.0 −252111.6 C 6 6 23 PHR0730−2151 236.7−01.6 073046.9 −215143.9 C 3 6 24 ESO427−19 239.6−12.0 065512.1 −290728.4 C 3 6 25 NGC2610† 239.6+13.9 083323.5 −160855.9 E 13 7 26 PHR0726−2858 242.5−05.9 072604.8 −285823.5 C 4 7 27 PRTM1 243.8−37.1 050301.7 −394544.0 C 3 7 28 PHR0742−3247 247.5−04.7 074223.6 −324744.9 C 3 7 29 A23 249.3−05.4 074318.9 −344513.0 C 3 7 30 PHR0834−2819 249.8+07.1 083418.1 −281903.0 C 3 7 31 PHR0803−3331 250.4−01.3 080312.5 −333101.9 C 4 8 32 PHR0736−3901 252.4−08.7 073625.2 −390131.1 C 3 8 33 PHR0820−3516 253.9+00.7 082052.4 −351632.9 C 3 8 34 VBRC1 257.5+00.6 083058.0 −381952.3 C 3 8 35 Wray17−1 258.0−15.7 071448.0 −465724.4 C 3 8 36 He2−11 259.1+00.9 083708.2 −392625.5 C 3 8 37 Wray16−20 260.7−03.3 082340.4 −431244.0 C 3 9 38 He2−15 261.6+03.0 085330.6 −400334.4 C 3 9 39 NGC2818 261.9+08.5 091600.5 −363731.6 E 20 9 40 Wray17−18 262.6−04.6 082353.7 −453109.9 E 10 9 41 ESO209−15 263.3−08.8 080510.9 −482330.1 E 20 9 42 He2−7† 264.1−08.1 081131.9 −484314.5 C 3 9 43 ESO259−10 265.1−04.2 083407.0 −471638.1 C 3 10 44 PHR0911−4205 265.4+04.2 091148.5 −420509.9 C 4 10 45 PHR0927−4347 268.6+05.0 092728.1 −434753.2 C 6 10 46 PHR0905−4753 268.9−00.4 090539.6 −475338.0 C 3 10 47 He2−37 274.6+03.5 094724.3 −485819.1 C 3 10 48 PHR0924−5506 276.1−03.3 092415.1 −550624.8 C 6 10 49 NGC2899 277.1−03.8 092703.5 −560618.3 E 20 11 50 PHR0958−5039 277.1+03.3 095810.2 −503934.9 C 6 11 51 Wray17−31 277.7−03.5 093127.1 −561741.1 E 20 11 52 He2−32 278.5−04.5 093055.9 −573657.8 C 3 11 53 PHR0940−5658 279.1−03.1 094052.5 −565800.1 C 3 11 54 PHR1010−5146 279.2+03.5 101004.1 −514648.0 C 6 11 55 He2−36 279.6−03.1 094326.0 −571659.7 E 10 12 56 Ste 2−1 280.0+02.9 101157.9 −523815.2 C 3 12 57 PHR1019−6059 285.5−03.3 101927.6 −605909.9 C 3 12

Article number, page 35 of 36 A&A proofs: manuscript no. neb1

Table 4. continued.

N Name PNG RA(J2000) Dec(J2000) Telescope Images Figure 58 PHR1036−5909 286.3−00.7 103609.2 −590920.2 C 6 12 59 He2−55 286.3+02.8 104843.1 −560323.0 E 14 12 60 PHR1046−6109 288.4−01.8 104651.1 −610923.0 C 3 12 61 Hf38 288.4+00.3 105434.9 −590948.7 C 3 13 62 PHR1058−5853 288.7+00.8 105802.9 −585334.1 C 3 13 63 Hf39 288.9−00.8 105358.9 −602642.0 E 3 13 64 Hf48∗ 290.1−00.4 110355.6 −603605.6 E 20 13 65 Fg1 290.5+07.9 112835.9 −525606.4 E 10 13 66 NGC3699∗ 292.6+01.2 112759.2 −595732.0 C 3 13 67 He2−70∗ 293.6+01.2 113512.6 −601654.1 C 3 14 68 BlDz1 293.6+10.9 115303.8 −505041.8 E 25 14 69 NGC3918 294.6+04.7 115018.9 −571051.4 E 20 14 70 He2−72∗ 294.9−00.6 114137.9 −622856.9 C 3 14 71 NGC3195 296.6−20.0 100922.0 −805130.6 E 10 14 72 He2−76 298.2−01.7 120826.0 −641212.1 E 13 14 73 PHR1221−5907 299.0+03.5 122100.7 −590732.9 C 4 15 74 K1−23 299.0+18.4 123052.0 −441422.2 E 20 15 75 Wray16−121 302.6−00.9 124831.1 −634956.5 C 3 15 76 PHR1250−6346 302.7−00.9 125004.4 −634651.9 E 14 15 77 Wray16−122 304.2+05.9 130041.4 −565328.3 C 6 15 78 NGC5189∗ 307.2−03.4 133341.9 −655828.9 E 20 15 79 He2−99 309.0−04.2 135231.0 −662328.0 E 19 16 80 VBRC5 309.2+01.3 134359.2 −604940.4 C 3 16 81 He2−103 310.7−02.9 140536.9 −644057.0 E 20 16 82 LoTr7 310.8−05.9 141523.1 −673157.6 E 14 16 83 PHR1408−6229 311.7−00.9 140847.3 −622957.8 C 3 16 84 He2−111 315.0−00.3 143318.3 −604944.6 E 14 16 85 He2−119∗ 317.1−05.7 151039.9 −644019.1 E 20 17 86 VBRC6 317.8+03.3 144135.7 −561506.6 E 25 17 87 He2−114 318.3−02.0 150408.8 −605321.2 E 20 17 88 He2−116 318.3−02.5 150600.8 −612124.4 E 10 17 89 ESO135−04 318.4−03.0 150842.8 −614403.9 E 20 17 90 IC4406∗ 319.6+15.7 142226.5 −440906.0 E 10 17 91 He2−120 321.8+01.9 151156.1 −553951.1 E 10 18 92 Mz1 322.4−02.6 153416.7 −590859.5 E 10 18 93 He2−163 327.8−07.2 162930.3 −590922.3 E 12 18 94 He2−146 328.9−02.4 161040.9 −545731.9 E 20 18 95 Mz2 329.3−02.8 161432.1 −545704.0 E 20 18 96 PHR1557−5128 329.7+01.4 155707.4 −512800.8 E 20 18 97 He2−165 331.5−03.9 162959.6 −540936.7 E 12 19 98 He2−164 332.0−03.3 162953.2 −532304.1 E 14 19 99 IC4642 334.3−09.3 171145.4 −552402.4 E 10 19 100 Lo12 340.8+10.8 160826.3 −370848.3 E 20 19 101 NGC6153 341.8+05.4 163130.9 −401522.5 E 14 19 102 H1−3 342.7+00.7 165331.5 −423918.1 E 10 19 103 Pe1−8 342.9−02.0 170622.8 −441312.1 E 10 20 104 He2−207 342.9−04.9 171932.5 −455310.0 E 18 20 105 IC4637 345.4+00.1 170509.0 −405257.1 E 10 20 106 K1−3∗ 346.9+12.4 162317.3 −314456.9 E 12 20 107 K2−16† 352.9+11.4 164449.1 −280405.4 E 17 20 108 Wray16−411 353.7−12.8 182641.5 −402951.1 E 14 20

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